We also find that the emission region in all channels is significantly more compact than the corotation radius of 0.05 au and slightly smaller than the magnetospheric radius of 0.037 au estimated from stellar parameters and an assumed magnetic field strength of 1 kG. As most of the observational evidence actually suggests the magnetic field to be on the order of up to 1.5 kG (e.g, [1]}, [2]}, [3]}), we can adjust the estimate of the truncation radius to 0.046 au and still find it to be less extended, but close to the corotation radius, which is expected for magnetospheric accretion. This agreement and the compact nature of the Br\(\gamma \)  half flux region when compared to the corotation radius are making a compelling case for the idea that Br\(\gamma \)  emission in TW Hya indeed orginates from the magnetosphere. This is further supported by the size profile. The decrease in HWHM would be expected under a magnetospheric accretion scenario as line components with the highest velocity are likely tracing gas in free fall towards the stellar surface.
